1. The Neutrino Telescope of the KM3NeT Deep-Sea Research Infrastructure Robert Lahmann for the KM3NeT Consortium Erlangen Centre for Astroparticle Physics TIPP 2011, Chicago 11-June-2011

2. 2Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Outline Objectives and Physics Case Technical Design and Implementation Optical Modules and Electronics

3. 3Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Objectives and Physics Case Technical Design and Implementation Optical Modules and Electronics

4. 4Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 What is KM3NeT ? Future cubic-kilometre scale neutrino telescope in the Mediterranean Sea Exceeds Northern-hemisphere telescopes by factor ~100 in sensitivity Exceeds IceCube sensitivity by substantial factor Provides node for earth and marine sciences (continuous deep-sea measurements)

5. 5Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 KM3NeT Organisation The KM3NeT consortium:  40 European institutes including those from Antares, Nemo and Nestor neutrino telescope projects  10 countries (Cyprus, France, Germany, Greece, Ireland, Italy, The Netherlands, Rumania, Spain, U.K) TDR published: http://www.km3net.org/TDR/KM3NeT-TDR.pdf (ISBN 978-90-6488-033-9)

6. 6Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 South Pole and Mediterranean Fields of View > 75% > 25% 2  downward sensitivity assumed In Mediterranean, visibility of given source can be limited to less than 24h per day

7. 7Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 The Objectives Central physics goals: –Investigate neutrino “point sources” in energy regime 1-100 TeV –Complement IceCube field of view –Substantially exceed IceCube sensitivity –Topics not used for optimisation: -Dark Matter -Neutrino particle physics aspects -Exotics (Magnetic Monopoles, Lorentz invariance violation, …) Implementation requirements: –Construction time ≤5 years –Operation over at least 10 years without “major maintenance”

8. 8Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Objectives and Physics Case Technical Design and Implementation Optical Modules and Electronics

9. 9Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 KM3NeT in the Mediterranean Sea Long-term site characterisation measurements performed during the Design Study at three different locations: Toulon (ANTARES), Capo Passero (NEMO) Pylos area (NESTOR) Infrastructure of networked KM3NeT nodes foreseen

10. 10Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Objective: Support 3D-array of photodetectors and connect them to shore (data, power, slow control) –Optical Modules –Front-end electronics –Readout, data acquisition, data transport –Mechanical structures, backbone cable –General deployment strategy –Sea-bed network: cables, junction boxes –Calibration devices –Shore infrastructure –Assembly, transport, logistics –Risk analysis and quality control Technical Design Design rationale: Cost-effective Reliable Producible Easy to deploy Unique or preferred solutions

11. 11Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 The Deep Sea environment High pressure (~200bar at 2km) Salt water: highly corrosive environment Long distance from shore for communication Forces on structure due to sea currents Wet-mateable connectors required One of the most adverse places for a technical installation: Optical calibration: See poster #13 by U. Emanuele Acoustic position calibration: Acoustic Emitters Detection Unit Receiver

12. 12Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 6 m Detection unit (DU): 20 storeys / 40 m distance (DU height ~ 900 m) storey: bar of 6 m with 2 DOMs DOM: digital optical module with 31 3” PMT KM3NeT DU KM3NeT storey KM3NeT DOM DUSt/DUDOM/St.PMT/DOM PMT 154 20 2 31 190 960 KM3NeT “Building Block” configuration KM3Net Detection Unit Storey buoyancy (syntactic foam) Cable reel

13. 13Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011  Surface area =  R 2 = 4.2 km 2 R = 1160 m Instrumented volume =  R 2 h h = 760m (19x40) V inst ≈ 3 km 3 2 Building Blocks will make up KM3NeT Budget ~220 M€ Building Block: Currently considered option: Randomised hexagonial grid Detector Geometry

14. 14Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Data Network and Data Transmission All data to shore concept (no trigger undersea) Data transport on optical fibers (data, slow control) –Optical point-to-point connection DOM-shore  large number of channels –DWDM (Dense Wavelength Division Multiplexing) technique: signals carried by different frequencies (colors) over the same fibre  minimize number of fibers Alternative option: Ring geometry Star geometry of power and fibre distribution EOC = electro-optical cable MVC = main voltage converter PJB = primary junction box SJB = secondary junction box

15. 15Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Optical Network OFM OM 20½ DU PJB SJB e e Up tp ~80 λ / fibre < 10 Gbps P2P Up to ~70 fibres in main cable Time delay measurements possible APD REAM e e e SS APD e o Dense Wavelength Division Multiplexing: Following ITU Grid Specification: C (1530-1570 nm) or L band (1570-1610 nm) with 25GHz separation

16. 16Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Objectives and Physics Case Technical Design and Implementation Optical Modules and Electronics

17. 17Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Sphere  17” PMTs (19+12)  3” Base –Adjust. HV (800-1400V) –Comparator for time-over-threshold Power board, electronics Calibration devices Single penetrator 17 DOM (Digital Optical Module) Multi-PMT Design: Large photocathode area per OM Single vs. multi-photon hit separation

18. 18Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Photo Multiplier Tubes Requirements: Quantum efficiency (QE) at 404nm>32% (>20% @ 470nm) Transit time spread (TTS)<2ns (sigma) Gain 5x10 6 Prototype tubes from company ETEL: Requirements adapted to in-situ conditions: Cherenkov photon spectrum in Mediterranean Sea most intense between ~400nm and ~500nm Chromatic dispersion sets lower level of required TTS

19. 19Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 DOMs: Recent Technical Progress Concentrator ring Increases effective photocathode area by 20-40% Ring simplifies PMT fixture Normalisation

20. 20Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Front End Electronics Threshold 1 Threshold 2 Threshold 3 Time Amplitude t1t1 t2t2 t3t3 t4t4 t5t5 t6t6 Time-over-threshold (TOT): Two options for readout FPGA (system on chip) 31x “Scott chip” (ASIC) Analog signal Comparator LVDS signal TDC Time stamped “hits” TOT count (time stamp in FPGA) (levels set through I 2 C control) Scott = Sampler of Comparator Outputs with Time Tagging TDC = Time to Digital Converter Timing resolution of ~1ns required

21. 21Robert Lahmann – TIPP2011 workshop, Chicago, 11-June-2011 Summary and Conclusions Major technical design decisions taken, minor points optimised for mass production In-situ operation of prototype Detection Unit planned for first half of 2012 Footprint being optimised for detection of Galactic sources Infrastructure of networked KM3NeT nodes most likely scenario Data taking could start 2014 Funding provided by EU through FP6 contract no. 011937 and FP7 grant agreement no. 212252